Evidence for solar neutrino flux variability and its implications |
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| Institution: | 1. Physics Department, University of California, Santa Barbara, CA 93106-9530, USA;2. Center for Space Science and Astrophysics, Stanford University, Stanford, CA 94305-4060, USA;1. I.I. Schmalhausen Institute of Zoology of National Academy of Sciences of Ukraine, vul. Bogdana Khmelnitskogo 15, 01601 Kyiv, Ukraine;2. Institute of Parasitology of Slovak Academy of Sciences, Hlinkova 3, 04001 Ko?ice, Slovakia;3. W. Stefański Institute of Parasitology of Polish Academy of Sciences, Twarda 51/55, 00-818 Warsaw, Poland;4. Veterinary Private Practice, Mickiewicza 41, Pisz, Poland;5. Wroclaw University of Environmental and Life Sciences, Norwida 25/27, 50-375 Wroclaw, Poland;1. Key Laboratory of Dynamics and Control of Flight Vehicle, Ministry of Education, School of Aerospace Engineering, Beijing Institute of Technology, Beijing 100081, China;2. Department of Mechanical and Aerospace Engineering, University of Missouri, Columbia, MO, 65211, USA;1. ICC, University of Barcelona (UB-IEEC), Marti i Franques 1, 08028, Barcelona, Spain;2. ICREA, Pg. Lluis Companys 23, 08010 Barcelona, Spain;3. Radcliffe Institute for Advanced Study, Harvard University, MA 02138, USA;4. Institute for Theory & Computation, Harvard University, 60 Garden Street, Cambridge, MA 02138, USA;5. Instituto de Fisica Corpuscular, CSIC-UVEG, P.O. 22085, Valencia, 46071, Spain;6. Laboratorio Subterráneo de Canfranc, Estación de Canfranc, 22880, Spain;7. Institute of Theoretical Astrophysics, University of Oslo, Oslo, 0315, Norway |
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| Abstract: | Although KamLAND apparently rules out resonant-spin-flavor-precession (RSFP) as an explanation of the solar neutrino deficit, the solar neutrino fluxes in the Cl and Ga experiments appear to vary with solar rotation. Added to this evidence, summarized here, a power spectrum analysis of the Super-Kamiokande data reveals significant variation in the flux matching a dominant rotation rate observed in the solar magnetic field in the same time period. Three frequency peaks, all related to this rotation rate, can be explained quantitatively. A Super-Kamiokande paper reported no time variation of the flux, but showed the same peaks, there interpreted as statistically insignificant, due to an inappropriate analysis. This modulation is small (7%) in the Super-Kamiokande energy region (and below the sensitivity of the Super-Kamiokande analysis) and is consistent with RSFP as a subdominant neutrino process in the convection zone. The data display effects that correspond to solar-cycle changes in the magnetic field, typical of the convection zone. This subdominant process requires new physics: a large neutrino transition magnetic moment and a light sterile neutrino, since an effect of this amplitude occurring in the convection zone cannot be achieved with the three known neutrinos. It does, however, resolve current problems in providing fits to all experimental estimates of the mean neutrino flux, and is compatible with the extensive evidence for solar neutrino flux variability. |
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